Celestial hemisphere:  Northern  ·  Constellation: Cassiopeia (Cas)  ·  Contains:  LBN 592  ·  LBN 593  ·  LDN 1282  ·  LDN 1283  ·  Sh2-173
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The Phantom of the Opera Nebula Sh2-173, Barry Wilson
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The Phantom of the Opera Nebula Sh2-173

Getting plate-solving status, please wait...
The Phantom of the Opera Nebula Sh2-173, Barry Wilson
Powered byPixInsight

The Phantom of the Opera Nebula Sh2-173

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Description

Resembling a character from the popular musical theatre The Phantom of the Opera Nebula in the constellation of Cassiopeia is a relatively faint emission nebula.  Controlling stars as you process the image is a challenge. There is an interesting paper on the nebula and its contribution to stellar formation, see Royal Astronomical Society:
"Based on a multiwavelength study, the interstellar medium around the H IIregion Sh2-173 has been analysed. The ionized region is clearly detected in the optical and the radio continuum images. The analysis of the H I data shows a region of low emissivity that has an excellent morphological correlation with the radio continuum emission. The H II region is partially bordered by a photodissociation region, which, in turn, is encircled by a molecular structure. The H I and CO structures related to Sh2-173 are observed in the velocity ranges from −25 to −31 km s−1 and from −27 to −39 km s−1, respectively. Taking into account the presence of non-circular motions in the Perseus spiral arm, together with previous distance estimates for the region, we adopt a distance of 2.5 ± 0.5 kpc for Sh2-173. Seven hot stars were identified in the field of Sh2-173, being only one O-type star. The amount of energetic photons emitted by this star is enough to keep the region ionized and heat the dust. Given that an expanding H II region may trigger star formation, a search for young stellar object (YSO) candidates was made using different infrared point source catalogues. A population of 46 YSO candidates was identified, projected on to the molecular clouds.On the other hand, Sh2-173 is located in a dense edge of a large (∼5°) H I shell, GSH 117.8+1.5-35. The possibility of Sh2-173 being part of a hierarchical system of three generations is suggested. In this scenario, the large H I shell, which probably originated due to the action of Cas OB5, would have triggered the formation of Sh2-173, which, in turn, is triggering new stars in its surrounding molecular cloud. To test this hypothesis, the ages of both the H II region and the large shell were estimated and compared. We concluded that Sh2-173 is a young H II region of about 0.6–1.0 Myr old. As for the large shell, we obtained a dynamical age of 5 ± 1 Myr. These age estimates, together with the relative location of the different structures, support the hypothesis that Sh2-173 is part of a hierarchical system."

Data acquisition: Barry Wilson & Steve Milne
Processing: Barry Wilson

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